J/A+A/645/A142 SDC G335.579-0.292 ALMA images and datacubes (Avison+, 2021)
Continuity of accretion from clumps to Class 0 high-mass protostars in SDC335.
Avison A., Fuller G.A., Peretto N., Duarte-Cabral A., Rosen A.L.,
Traficante A., Pineda J.E., Gusten R., Cunningham N.
<Astron. Astrophys. 645, A142 (2021)>
=2021A&A...645A.142A 2021A&A...645A.142A (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Protostars ; Spectra, millimetric/submm
Keywords: stars: formation - ISM: jets and outflows - stars: massive -
stars: protostars - ISM: clouds - masers
Abstract:
The infrared dark cloud (IRDC) SDC335.579-0.292 (hereafter, SDC335)
is a massive (∼5000 solar masses) star-forming cloud which has been
found to be globally collapsing towards one of the most massive star
forming cores in the Galaxy, which is located at its centre. SDC335 is
known to host three high-mass protostellar objects at early stages of
their evolution and archival ALMA Cycle 0 data (at ∼5 arcsecond
resolution) indicate the presence of at least one molecular outflow in
the region detected in HNC. Observations of molecular outflows from
massive protostellar objects allow us to estimate the accretion rates
of the protostars as well as to assess the disruptive impact that
stars have on their natal clouds during their formation. The aim of
this work is to identify and analyse the properties of the
protostellar-driven molecular outflows within SDC335 and use these
outflows to help refine the properties of the young massive protostars
in this cloud. We imaged the molecular outflows in SDC335 using new
data from the Australia Telescope Compact Array (ATCA) of SiO and
Class I CH3OH maser emission (at a resolution of ∼3 arcsecond)
alongside observations of four CO transitions made with the Atacama
Pathfinder EXperiment (APEX) and archival Atacama Large
Millimeter/submillimeter Array (ALMA) CO, 13CO (∼1 arcsecond), and HNC
data. We introduced a generalised argument to constrain outflow
inclination angles based on observed outflow properties. We then used
the properties of each outflow to infer the accretion rates on the
protostellar sources driving them. These accretion properties allowed
us to deduce the evolutionary characteristics of the sources.
Shock-tracing SiO emission and CH3OH Class I maser emission allowed
us to locate regions of interaction between the outflows and material
infalling to the central region via the filamentary arms of SDC335.
Description:
Molecular line data cubes (RA, Dec, Velocity) of CO, 13CO and HNC
observed with ALMA and SiO and CH3OH observed using the Australia
Telescope Compact Array (ATCA).
Objects:
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RA (2000) DE Designation(s)
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16 30 58.00 -48 44 16.3 SDC 335 = SDC G335.579-0.292
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
listsp.dat 59 12 List of spectra
spectra/* . 12 Individual molecular line spectra of outflows
list.dat 136 20 List of fits images and datacubes
fits/* . 20 Individual fits images and datacubes
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Byte-by-byte Description of file: listsp.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 25 A25 --- FileName Name of the file in subdirectory spectra
27- 59 A33 --- Title Title of the file
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Byte-by-byte Description of file: spectra/*
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Bytes Format Units Label Explanations
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1- 19 E19.11 km/s Vel Radio Velocity of channel
21- 40 E20.11 Jy/beam S Mean flux density (1)
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Note (1): Spectra in the spectra subdirectory are as observed within a polygon
region around each outflow. Exact polygons are available from the author upon
request.
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 2 I2 h RAh Right Ascension (J2000) of image center
4- 5 I2 min RAm Right Ascension (J2000) of image center
7- 12 F6.3 s RAs Right Ascension (J2000) of image center
14 A1 --- DE- Declination sign (J2000) of image centre
15- 16 I2 deg DEd Declination (J2000) of image centre
18- 19 I2 arcmin DEm Declination (J2000) of image centre
21- 25 F5.2 arcsec DEs Declination (J2000) of image centre
27- 29 I3 --- Nx Number of pixel along X-axis
31- 33 I3 --- Ny Number of pixel along Y-axis
35- 37 I3 --- Nz ? Number of slices for the datacubes
39- 41 F3.1 arcsec/pix scale Pixel scale in the image
43- 48 F6.4 MHz scaleC ? Channel width in the Cube z axis
50- 62 E13.7 Hz ObsFreq ? Rest frequency of observations
for the datacubes
64- 69 I6 Kibyte size Size of FITS file
71- 95 A25 --- FileName Name of FITS file in subdirectory fits
97-136 A40 --- Title Title of the file
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Acknowledgements:
Adam Avison, adam.avison(at)manchester.ac.uk
(End) Patricia Vannier [CDS] 09-Dec-2020